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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/1192
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dc.contributor.authorArun, K.G.-
dc.contributor.authorIyer, B.R.-
dc.contributor.authorSathyaprakash, B.S.-
dc.contributor.authorSundarajan, P.A.-
dc.date.accessioned2006-05-12T04:28:29Z-
dc.date.available2006-05-12T04:28:29Z-
dc.date.issued2005-04-06-
dc.identifier.citationPhysical Review D, 2005, Vol.71, 084008en
dc.identifier.issn1550-7998-
dc.identifier.issn1550-2368 (online)-
dc.identifier.urihttp://hdl.handle.net/2289/1192-
dc.description.abstractWe revisit the problem of parameter estimation of gravitational-wave chirp signals from inspiralling nonspinning compact binaries in the light of the recent extension of the post-Newtonian (PN) phasing formula to order (v/c)7 beyond the leading Newtonian order. We study in detail the implications of higher post-Newtonian orders from 1PN up to 3.5PN in steps of 0.5PN (~v/c), and examine their convergence. In both initial and advanced detectors the estimation of the chirp mass ([script M]) and symmetric mass ratio (eta) improve at higher PN orders but oscillate with every half-a-PN order. In initial LIGO, for a 10M[sun]–10M[sun] binary at a signal-to-noise ratio (SNR) of 10, the improvement in the estimation of [script M] (eta) at 3.5PN relative to 2PN is ~19% (52%). We compare parameter estimation in different detectors and assess their relative performance in two different ways: at a fixed SNR, with the aim of understanding how the bandwidth improves parameter estimation, and for a fixed source, to gauge the importance of sensitivity. Errors in parameter estimation at a fixed SNR are smaller for VIRGO than for both initial and advanced LIGO. This is because of the larger bandwidth over which it observes the signals. However, for sources at a fixed distance it is advanced LIGO that achieves the lowest errors owing to its greater sensitivity. Finally, we compute the amplitude corrections due to the "frequency-sweep" in the Fourier domain representation of the waveform within the stationary phase approximation and discuss its implication on parameter estimation. We find that the amplitude corrections change the errors in [script M] and eta by less than 10% for initial LIGO at a signal-to-noise ratio of 10. Our analysis makes explicit the significance of higher PN order modeling of the inspiralling compact binary on parameter estimation.en
dc.format.extent228023 bytes-
dc.format.extent39530 bytes-
dc.format.mimetypeapplication/pdf-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherThe American Physical Societyen
dc.relation.urihttp://link.aps.org/abstract/PRD/v71/e084008en
dc.relation.urihttp://arxiv.org/abs/gr-qc/0411146-
dc.rights(2005) by the American Physical Societyen
dc.titleParameter estimation of inspiralling compact binaries using 3.5 post-Newtonian gravitational wave phasing: The nonspinning caseen
dc.typeArticleen
dc.additionalErratum published in Physical Review D, Vol.72, 06993(E), 2005.en
Appears in Collections:Research Papers (TP)

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